An Introduction to Mean Field Dynamo Theory
Chapter 2 An Introduction to Mean Field Dynamo Theory D.W. Hughes and S.M. Tobias Department of Applied Mathematics, University of Leeds 2.1 Introduction Magnetic fields are essentially ubiquitous, being detected over a tremen dous range of scales in planets, stars, accretion discs and in the interstellar medium. The dynamic behaviour of such fields is then responsible for a vast range of astrophysical phenomena (see, for example, Parker 1979). For instance, the solar magnetic field gives rise to sunspots, solar flares and coronal mass ejections; it also plays a major role in shaping the solar wind which, on interacting with the Earth's magnetic field, causes auro rae. Starspots, analogous to sunspots but covering a much greater surface area, have been detected on a number of cool stars. The pulsed emission of pulsars is a consequence of an extremely strong magnetic field. On the largest scales, the interstellar magnetic field plays a role in star formation, mediating angular momentum transport as the star collapses. The ulti mate question in the 'study of astrophysical magnetic fields must then be that of the origin of the magnetic field in cosmical objects. In particu lar, one might ask whether the observed magnetic fields are simply 'fossil fields', or whether, alternatively, they are being continually regenerated - i.~. whether some sort of dynamo process is taking place. For collision-dominated plasmas with short mean free paths, such as those found in stellar interiors, the evolution of magnetic fields is very well described by the equations of single-fluid magnetohydrodynamics (MHD). 15 16 Relaxation Dynamics in Laboratory and Astrophysical Plasmas (Although, for example, in studies of stellar atmospheres - such as the solar corona - the use of MHD is not based on such solid foundations.) In this review we shall be concerned only with physical systems for which the MHD description is appropriate.
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